For what concerns RU Lup's accretion variability, long-term photometric monitoring by [1]} already showed stochastic variability and lack of a single stable periodic pattern in its light-curves. The authors inferred that an unstable accretion regime, typical of CTTSs with high-mass accretion rates, operates in RU Lup. In particular, they argue that RU Lup's photometric variability is due to increased mass accretion rates that can prompt Rayleigh–Taylor (RT) instabilities, moving accretion from a stable to an unstable regime, as predicted by several 3D MHD simulations of disk accretion onto a rotating
magnetised star [2]}, [3]}, [4]}.
